论文标题
从Young Massive Star Cluster RSGC 1附近的弥漫性伽马射线排放1
Diffuse gamma-ray emission from the vicinity of young massive star cluster RSGC 1
论文作者
论文摘要
我们报告了Fermi大面积望远镜（Fermi-LAT）检测对年轻的大型巨星群集RSGC 1的伽马射线发射。使用最新的源目录和弥漫性背景模型，我们发现该区域的弥漫性伽马射线发射可以分辨为三种不同的组件。 HESS J1837-069地区的GEV伽马射线排放的光子指数为1.83 $ \ pm $ 0.08。与HESS和魔术数据相结合，我们认为该地区的伽马射线发射可能起源于脉冲星云（PWN）。西北部（区域A）的伽马射线排放可以通过椭圆形成0.5 $^{\ circ} $和0.25 $^{\ circ} $的椭圆形。 GEV排放具有硬光谱，光子指数为2.05 $ \ pm $ 0.02，并且与TEV Source Magic J1835-069的部分相吻合。该区域中伽马射线发射的可能起源是由SNR G24.7+0.6或/和OB簇G25.18+0.26与周围气体云加速的宇宙射线（CRS）相互作用。东南地区（B区）的GEV伽马射线发射可以分别以0.9 $^{\ Circ} $和0.5 $^{\ Circ} $的半轴和半轴轴建模，并且还显示了硬γ射线光谱。我们认为，最可能的起源是年轻的巨大星团RSGC 1与环境气云中加速质子的相互作用，估计总宇宙射线（CR）质子能量高达$ \ sim $ 1x10 $^{50} $ ERG。
We report the Fermi Large Area Telescope (Fermi-LAT) detection of the gamma-ray emission towards the young massive star cluster RSGC 1. Using the latest source catalog and diffuse background models, we found that the diffuse gamma-ray emission in this region can be resolved into three different components. The GeV gamma-ray emission from the region HESS J1837-069 has a photon index of 1.83 $\pm$ 0.08. Combining with the HESS and MAGIC data, we argue that the gamma-ray emission in this region likely originate from a pulsar wind nebula (PWN). The gamma-ray emission from the northwest part (region A) can be modelled by an ellipse with the semimajor and semiminor axis of 0.5$^{\circ}$ and 0.25$^{\circ}$, respectively. The GeV emission has a hard spectrum with a photon index of 2.05 $\pm$ 0.02 and is partially coincide with the TeV source MAGIC J1835-069. The possible origin of the gamma-ray emission in this region is the interaction of the cosmic rays (CRs) accelerated by SNR G24.7+0.6 or/and the OB cluster G25.18+0.26 with the surrounding gas clouds. The GeV gamma-ray emission from the southeast region (region B) can be modeled as an ellipse with the semimajor and semiminor axis of 0.9$^{\circ}$ and 0.5$^{\circ}$, respectively, and also reveals a hard gamma-ray spectrum. We argue that the most probable origin is the interaction of the accelerated protons in the young massive star cluster RSGC 1 with ambient gas clouds, and the total cosmic-ray (CR) proton energy is estimated to be as high as $\sim$ 1x10$^{50}$ erg.
